Göttingen 2025 – wissenschaftliches Programm
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EP: Fachverband Extraterrestrische Physik
EP 15: Astrophysics III
EP 15.2: Vortrag
Freitag, 4. April 2025, 14:00–14:15, ZHG101
Time-dependent modeling of radiative processes in pulsar wind nebulae generated by neutron-star mergers — •Eric Schneider1, Michael Müller1, and Daniel Siegel1,2 — 1Institute of Physics, University of Greifswald, Greifswald, Germany — 2Department of Physics, University of Guelph, Guelph, Ontario, Canada
Emission from pulsar wind nebulae (PWNe) and the thermal emission of kilonovae (KN) have traditionally been studied as separate phenomena, associated with distinct astrophysical origins. A pulsar wind nebula is composed of a relativistic leptonic plasma powered by a pulsar typically found in supernova remnants. The leptons cool down through a variety of radiative processes, giving rise to distinct non-thermal emission. A KN is a thermal electromagnetic transient driven by the radioactive decay of neutron-rich nuclei, which are synthesized by the rapid neutron-capture process in the dense plasma outflows from neutron star mergers.
Recent models suggest PWNe may also form in binary neutron star mergers, driven by long-lived remnant neutron stars. These PWNe differ from their supernova counterparts because of their high compactness and high photon densities, requiring new theoretical approaches.
We present a unified model for PWNe evolution and electromagnetic emission, together with a generalized KN model that incorporates the presence of a PWN. We generate a catalog of combined non-thermal and thermal emission to aid interpretation of future merger observations and to constrain properties of merger remnants.
Keywords: Binary Neutron star mergers; Pulsar Wind Nebulae; Kilonovae; Gravitational waves; High energy astrophysics